*The Coronal Temperature and Polarization Experiment The Coronal Temperature and Polarization Experiment consists of a series of observations of the solar corona through three narrow bandpass filters and three polarizers. These observations allow us to create temperature, polarization angle, and polarization intensity maps of the corona. *Temperature and Polarization Experiment Scientific Objectives The main scientific objectives of this experiment were to produce maps of the coronal temperature, polarization angle, and polarization intensity. The polarization measurements are of particular importance because of our collaboration with the Ultraviolet Coronagraph Spectrometer (UVCS) team at the Harvard-Smithsonian Center for Astrophysics. *UVCS Collaboration The Ultraviolet Coronagraph Spectrometer (UVCS) and the Large Angle and Spectrometric Coronagraph (LASCO) -- both instruments aboard the SOHO spacecraft -- are capable of measuring the polarization of coronal light. The measurements made by the two instruments have been in disagreement, and our observations may help resolve the conflict. *Observations and Analysis Using a Meade 10" Schmidt-Cassegrain telescope, dual filter wheels, and a Princeton Instruments VersArray CCD camera, we took 23 exposures of the northwest quadrant of the corona through filters centered on 3875, 4050, and 4410 angstroms, and three polarizing filters oriented at 45 degree intervals. We used the remaining time of totality to take four exposures of Jupiter through a neutral density filter for calibration purposes. The coronal temperature maps are produced by analyzing the ratios of coronal intensity at various wavelengths. The ratios can be compared to theoretical calculations of the coronal spectrum that describe its dependence on temperature. The polarization maps are produced by comparing the images taken through the three polarizing filters, oriented at 45 degree intervals. It is well established that light scattered by coronal electrons is radially polarized with respect to the position of the sun, so the more important map is of the polarization intensity. *pictures: include two line plots, the annotated picture, maybe a coronal spectrum.